The 2001 April Burst Activation of SGR 1900+14: Pulse Properties and Torque

Woods, P. M.; Kouveliotou, C.; Göǧüş, E.; Finger, Mark H.; Feroci, M.; Mereghetti, S.; Swank, J. H.; Hurley, K.; Heise, J.; Smith, D. A.; Frontera, F.; Guidorzi, C.; Thompson, Christopher

doi:10.1086/376891

Cited by 17 publications

(22 citation statements)

References 31 publications

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“…We focus on three possibilities: first, no huge energy release comparable to that of GF98 occurred; second, the spiking event occurred, but the beamed outflow was not directed toward our line of sight; third, a comparable or slightly less energetic release really occurred, but the permanent changes undergone by the magnetosphere after the global reconfiguration further to GF98 are responsible for the unusual time profile of IF01. The first explanation seems the most natural, since it easily accounts for the lower X-and γ-ray fluence of IF01 and seems to agree with the minor changes observed in the trend of the pulsation profile after the flare against what occurred after GF98 (Gögüş et al 2002;Woods et al 2003). However the light curve of IF01 shows some similarities (e.g., dips at the same phase in the correspondence case of Fig.…”

Section: Light Curvesmentioning

confidence: 54%

“…4) to the initial stage of GF98. Furthermore, the pulse profile during IF01 appears far more complex than it appeared at the later stages of GF98 (Mazets et al 1999b) and than that of the quiescent pulsar after 1998 (Gögüş et al 2002;Woods et al 2003). This suggests that a transient reconfiguration of the magnetic field took place related to this event, that caused the complex pulse profile evolution during the burst.…”

Section: Light Curvesmentioning

confidence: 96%

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Comparative study of the two large flares from SGR1900+14 with theBeppoSAXGamma-Ray Burst Monitor

Guidorzi

Frontera

Montanari

et al. 2004

A&A

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Abstract. We report on spectral and temporal results of the 40-700 keV observations, obtained with the Gamma-Ray Burst Monitor (GRBM) on board BeppoSAX, of the two large flares from the Soft Gamma-ray Repeater SGR 1900+14 occurred on August 27, 1998 and April 18, 2001. From their intensity, fluence and duration, the first one was classified as "giant" and the second as "intermediate".The spectral results have been obtained with an improved response function of the GRBM. We find that the two events have similar spectral properties, but different temporal properties. The major difference concerns the time profiles of the light curves, whereas the lack of evidence in the 2001 flare for the erratic time variability found at high frequencies (10-1000 Hz) in the 1998 flare could be ascribed to lower counting statistics. We discuss these results in the light of the magnetar model proposed for SGR sources.

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Section: Light Curvesmentioning

confidence: 54%

Section: Light Curvesmentioning

confidence: 96%

Comparative study of the two large flares from SGR1900+14 with theBeppoSAXGamma-Ray Burst Monitor

Guidorzi

Frontera

Montanari

et al. 2004

A&A

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“…11 The power-law index of the flux decay ( § 3) falls within the range of those of SGRs (0.47-0.9); however, no SGR-like bursts were detected from the source. With the 11 See, e.g., SGR 1900ϩ14 (Woods et al 2001;Ibrahim et al 2001;Feroci et al 2003), 1E 2259ϩ586 (Kaspi et al 2003;Woods et al 2003), and SGR 1627Ϫ41 (Kouveliotou et al 2003). IPN, five bursts were recorded on 2002 December 5-6 (Hurley et al 2002).…”

Section: Discussionmentioning

confidence: 99%

Discovery of a Transient Magnetar: XTE J1810-197

Ibrahim

Markwardt

Swank

et al. 2004

ApJ

227

261

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We report the discovery of a new X-ray pulsar, XTE J1810Ϫ197, that was serendipitously discovered on 2003 July 15 by the Rossi X-Ray Timing Explorer (RXTE) while observing the soft gamma repeater SGR 1806Ϫ20. The pulsar has a 5.54 s spin period, a soft X-ray spectrum (with a photon index of ≈4), and is detectable in earlier RXTE observations back to 2003 January but not before. These show that a transient outburst began between 2002 November 17 and 2003 January 23 and that the source's persistent X-ray flux has been declining since then. The pulsar exhibits a high spin-down rate s s Ϫ1 with no evidence of Doppler shifts due to Ϫ11 P ≈ 10 a binary companion. The rapid spin-down rate and slow spin period imply a supercritical characteristic magnetic field G and a young age yr. Follow-up Chandra observations provided an accurate 14 B Ӎ 3 # 10 t ≤ 7600 position of the source. Within its error radius, the 1.5 m Russian-Turkish Optical Telescope found a limiting magnitude . All such properties are strikingly similar to those of anomalous X-ray pulsars and soft R p 21.5 C gamma repeaters, providing strong evidence that the source is a new magnetar. However, archival ASCA and ROSAT observations found the source nearly 2 orders of magnitude fainter. This transient behavior and the observed long-term flux variability of the source in absence of an observed SGR-like burst activity make it the first confirmed transient magnetar and suggest that other neutron stars that share the properties of XTE J1810Ϫ197 during its inactive phase may be unidentified transient magnetars awaiting detection via a similar activity. This implies a larger population of magnetars than previously surmised and a possible evolutionary connection between magnetars and other neutron star families.

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“…This event, which prompted the two following BeppoSAX observations (Feroci et al 2003(Feroci et al , 2004Woods et al 2003), had a duration of ∼40 s and a total fluence of 1.6 × 10 −4 erg cm −2 . Another bright flare, but of comparatively smaller fluence (∼9 × 10 −6 erg cm −2 ), occurred after 10 days (Lenters et al 2003).…”

Section: Sgr 1900+14: Activity Episodes and Bepposax Observationsmentioning

confidence: 94%

Five years of SGR 1900+14 observations withBeppoSAX

Esposito

Mereghetti

Tiengo

et al. 2006

A&A

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We present a systematic analysis of all the BeppoSAX data of the soft gamma-ray repeater SGR 1900+14: these observations allowed us to study the long term properties of the source quiescent emission. In the observation carried out before the 1998 giant flare the spectrum in the 0.8-10 keV energy range was harder and there was evidence for a 20-150 keV emission, possibly associated with SGR 1900+14. This possible hard tail, if compared with the recent INTEGRAL detection of SGR 1900+14, has a harder spectrum (power-law photon index ∼1.6 versus ∼3) and a 20-100 keV flux ∼4 times larger. In the last BeppoSAX observation (April 2002), while the source was entering the long quiescent period that lasted until 2006, the 2-10 keV flux was ∼25% below the historical level. We also studied in detail the spectral evolution during the 2001 flare afterglow. This was characterized by a softening that can be interpreted in terms of a cooling blackbody-like component.

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The 2001 April Burst Activation of SGR 1900+14: Pulse Properties and Torque

Cited by 17 publications

References 31 publications

Comparative study of the two large flares from SGR1900+14 with theBeppoSAXGamma-Ray Burst Monitor

Comparative study of the two large flares from SGR1900+14 with theBeppoSAXGamma-Ray Burst Monitor

Discovery of a Transient Magnetar: XTE J1810-197

Five years of SGR 1900+14 observations withBeppoSAX

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